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\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Active}
& \multicolumn{1}{|c|}{\large\em An electronic publication dedicated to}\\ [0.3cm]
\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Galaxies} & \multicolumn{1}{|c|}{\large\em the observation and theory of}\\ [0.3cm]
\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Newsletter} & \multicolumn{1}{|c|}{\large\em active galaxies}\\ [0.3cm]
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\multicolumn{1}{|c|}{\large\bf\sf No. 91 --- October 2004 } &
\multicolumn{1}{|c|}{\bf\sf Editor: Rob Beswick (rb@ast.man.ac.uk)} \\ [-0.1cm]
& \\ \hline
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\small
\begin{center}
{\Large\em Abstracts - Thesis Abstracts - Jobs - Meetings}
\end{center}
\begin{center}
{\Large\sf From the Editor}
\end{center}
\vspace*{0.6cm}
The Active Galaxies Newsletter is produced monthly. The deadline for
contributions is the last friday of the month. The Latex macros for
submitting abstracts and dissertation abstracts are appended to each
issue of the newsletter and are also available on the web page.
\newline Rob Beswick
\vspace*{1cm}
\begin{center}
{\Large\sf Abstracts of recently accepted papers}
\end{center}
\vspace*{0.6cm}
{\large\bf{Physical Conditions in the Narrow-Line Region of Markarian 3.
I. Observational Results}}
{\bf{Nicholas R. Collins$^1$, Steven B. Kraemer$^1$,
D. Michael Crenshaw$^2$, Jose Ruiz$^1$,\newline
Rajesh Deo$^2$ and Frederick C. Bruhweiler$^1$}}
$^1$ {Institute for Astrophysics and Computational
Sciences, Catholic University of America; \newline and NASA Goddard Space
Flight Center, Code 681, Greenbelt, MD 20771} \\
$^2$ {Department of Physics
and Astronomy, Georgia State University, Astronomy Offices,\newline
One Park Place South SE, Suite 700, Atlanta, GA 30303} \\
{We use Hubble Space Telescope/Space Telescope Imaging Spectrograph (HST/STIS)
longslit low-resolution spectroscopy from 1150~\AA~ to 10,300~\AA~ to study the
physical conditions in the narrow-line region (NLR) of the Seyfert~2 galaxy
Markarian~3. We find from the HeII~$\lambda$1640/$\lambda$4686 line ratio and
the Balmer decrement that the extinction within Markarian~3 along the
line-of-sight to the NLR is best characterized by a Large Magellanic Cloud (LMC)
type extinction curve. We observe an extinction gradient increasing from west to
east along the STIS slit (at position angle 71~degrees measured east from north)
in both line and continuum emission. We infer from this gradient that the host
galaxy disk is tilted towards the observer in the east: the line-of-sight to the
eastern emission-line cone intersects more dust in the plane of the galaxy than
that to the western cone. From emission-line diagnostics we find that the NLR
gas is photoionized by the hidden active galactic nucleus (AGN) continuum and
that its density decreases with increasing distance from the center. We model
the observed continuum as a combination of reddened host galaxy light from an old
stellar population, reddened H$^{+}$ and He$^{+2}$ recombination continua, and
less reddened scattered light from the central engine with spectral index
$\alpha$=1 (L$_{\nu}\propto\nu^{-\alpha}$). The host galaxy to scattered-light
ratio is estimated to be 3:1 at 8125~\AA~ in 0.1 $\times$ 1.8~square-arcsecond
aperture. Using a two-component power-law model for the ionizing continuum
($\alpha$=2 for 13.6~eV~$$0.7\%. We estimate that the amount of
intrinsic non-ionizing UV continuum scattered into our line-of-sight is 0.04\%.
This is consistent with our estimate of the scattering fraction for broad
CIV~$\lambda\lambda$1548,1551 emission.}
{ Accepted by ApJ }
{ E-mail contact: nicholas.r.collins.1@gsfc.nasa.gov }
\newpage
\newcommand{\gtrsim}{\stackrel{\scriptscriptstyle >}{\scriptstyle{}_\sim}}
{\large\bf{The Fundamental Plane Evolution of Active Galactic Nucleus Host
Galaxies}}
{\bf{Jong-Hak Woo$^1$, C. Megan Urry$^2$, Paulina Lira$^3$, Roeland P. van der
Marel$^4$ \ and Jose Maza$^5$ }}
$^1$ {Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT
06520-8101} \\
$^2$ {Department of Physics and Yale Center for Astronomy and Astrophysics, Yale
University, P.O. Box 208121, New Haven, CT 06520-8121 } \\
$^3$ {Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago,
Chile } \\
$^4$ { Space Telescope Science Institute, 3700 San Martin Dr. Baltimore MD 21218
} \\
$^5$ { Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago,
Chile }
{We measured the stellar velocity dispersions of 15 active galactic nucleus (AGN)
host galaxies at redshifts as high as $\sim 0.34$. Combining these with published
velocity dispersion measurements from the literature,we study the Fundamental
Plane of AGN host galaxies and its evolution. BL Lac hosts and radio galaxies
seem to lie on the same Fundamental Plane as normal early-type galaxies. The
evolution of the mass-to-light ratio of AGN host galaxies shows a similar trend
to that observed in normal early-type galaxies, consistent with single-burst
passive evolution models with formation redshifts $z \gtrsim 1$. The lack of a
significant difference between normal and AGN host galaxies in the Fundamental
plane supports the ``Grand Unification" picture wherein AGNs are a transient
phase in the evolution of normal galaxies. The black hole masses of BL Lac
objects and radio galaxies, derived using the mass -- dispersion relation, are
similar. The black hole mass is independent of BL Lac type. The local black hole
mass -- host galaxy luminosity relation of our sub-sample at $z < 0.1$ is similar
to that of local normal and radio galaxies, but is less well defined at higher
redshiftdue to the luminosity evolution of the host galaxies.}
{ Accepted by Astrophysical J.}
{E-mail contact: jhwoo@astro.yale.edu,\newline preprint available at
http://arxiv.org/abs/astro-ph/0409006}
\vspace*{0.6cm}
{\large\bf{Continuum Acceleration of Black Hole Winds}}
{\bf{John E. Everett and David R. Ballantyne}}
{Canadian Institute for Theoretical Astrophysics, University of
Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada}
{Motivated by recent observations of high-velocity, highly ionized winds in
several QSOs, models of purely continuum-driven winds launched from
$\sim200GM_{\rm BH}/c^2$ are presented. Launching conditions are investigated,
as well as the observational signatures for a variety of initial conditions and
illuminating continua. While we verify that continuum-driven highly ionized
outflows reach the observed velocities for $L/L_{\rm Edd}\geq1$ independent of
the incident spectral shape, such winds are too highly ionized to exhibit the
observed absorption features when launched with an active galactic nucleus
continuum (in fact, such winds are so ionized that they are driven primarily by
electron scattering). If the wind is instead illuminated with a blackbody
continuum originating from an optically thick shield, the gas is too weakly
ionized and does not produce high-energy absorption features. If high-velocity
high-ionization winds are truly launched from very near the black hole, such
winds must be launched under other conditions or via other processes; we
summarize some possibilities.}
{Accepted by ApJL }
{E-mail contact: everett@cita.utoronto.ca,\newline preprint available at
http://arxiv.org/abs/astro-ph/0409409}
\vspace*{0.6cm}
{\large\bf{Unveiling the nature of the highly obscured AGN in NGC~5643 with
XMM-Newton}}
{\bf{ M.~Guainazzi$^1$, P.~Rodriguez-Pascual$^1$, A.C.~Fabian$^2$,
K.~Iwasawa$^2$, and G.~Matt$^3$ }}
$^1$ {European Space Astronomy Center, RSSD of ESA, VILSPA, Apartado 50727,
E-28080 Madrid, Spain} \\
$^2$ {Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA} \\
$^3$ {Dipartimento di Fisica ``E.Amaldi", Universit\`a ``Roma Tre", Via della
Vasca Navale 84, I-00146 Roma, Italy}
{We present results from an XMM-Newton observation of the nearby Seyfert~2 galaxy
NGC~5643. The nucleus exhibits a very flat X-ray continuum above 2~keV, together
with a prominent K$_{\alpha}$ fluorescent iron line. This indicates heavy
obscuration. We measure an absorbing column density $N_H$ in the range
6--10$\times 10^{23}$~cm$^{-2}$, either directly covering the nuclear emission,
or covering its Compton-reflection. In the latter case, we might be observing a
rather unusual geometry for the absorber, whereby reflection from the inner far
side of a torus is in turn obscured by its near side outer atmosphere. The
nuclear emission might be then either covered by a Compton-thick absorber, or
undergoing a transient state of low activity. A second source (christened "X-1"
in this paper) at the outskirts of NGC~5643 optical surface outshines the nucleus
in X-rays. If belonging to NGC~5643, it is the third brightest ($L_X \sim 4
\times 10^{40}$~erg~s$^{-1}$) known Ultra Luminous X-ray source. Comparison with
past large aperture spectra of NGC~5643 unveils dramatic X-ray spectral changes
above 1~keV. We interpret them as due to variability of the active nucleus {\it
and} of source X-1 intrinsic X-ray powers by a factor $\ge$10 and 5,
respectively.}
{ Accepted by MNRAS }
{E-mail contact: Matteo.Guainazzi@sciops.esa.int,\newline preprint available at
or http://arxiv.org/abs/astro-ph/0408300}
\vspace*{0.6cm}
{\large\bf{The Largest Blueshifts of [O III] emission line in Two Narrow-Line
Quasars}}
{\bf{Kentaro Aoki$^1$, Toshihiro Kawaguchi$^2$ \ and Kouji Ohta$^3$ }}
$^1$ {Subaru Telescope, National Astronomical Observatory of Japan,
650 North A'ohoku Place, Hilo, HI 96720 U.S.A.} \\
$^2$ {LUTH, Observatoire de Paris, Section de Meudon, 5 Place J. Janssen, 92195
Meudon, France} \\
$^3$ {Department of Astronomy, Kyoto University, Kyoto 606-8502, Japan}
{We have obtained optical intermediate resolution spectra ($R$ = 3000) of the
narrow-line quasars DMS 0059$-$0055 and PG 1543+489. The [O III] emission line in
DMS 0059$-$0055 is blueshifted by 880 km s$^{-1}$ relative to H$\beta$. We also
confirm that the [O III] emission line in PG 1543+489 has a relative blueshift of
1150 km s$^{-1}$. These two narrow-line quasars show the largest [O III]
blueshifts known to date among type 1 active galactic nuclei (AGNs). The [O III]
emission lines in both objects are broad (1000 -- 2000 km s$^{-1}$) and those in
DMS 0059$-$0055 show strong blue asymmetry. We interpret the large blueshift and
the profile of the [O III] lines as the result of an outflow interacting with
circumnuclear gas. Among type 1 AGNs with large blueshifted [O III], there is no
correlation between the Eddington ratios and the amount of [O III] blueshifts.
Combining our new data with published results, we confirm that the Eddington
ratios of the such AGNs are the highest among AGNs with the same black hole
masses. These facts suggest that the Eddington ratio is a necessary condition or
the [O III] blueshifts weakly depend on the Eddington ratio. Our new sample
suggests that there are possible necessary conditions to produce an outflow
besides a high Eddington ratio: large black hole mass ($ > 10^{7} M_{solar}$) or
high mass accretion rate ($> 2 M_{solar}$/yr) or large luminosity ($\lambda
L_{\lambda} (5100 {\rm \AA}) > 10^{44.6}$ erg s$^{-1}$). }
{ Accepted for publication in The Astrophysical Journal. }
{E-mail contact: kaoki@subaru.naoj.org,\newline preprint available at
http://arxiv.org/abs/astro-ph/0409546}
\vspace*{0.6cm}
{\large\bf{Neutral hydrogen at milliarcsecond resolutions: The radio galaxy 3C293}}
{\bf{R.\,J.\,Beswick$^1$, A.\,B.\,Peck$^2$, G.\,B.\,Taylor$^3$, G. Giovannini$^4$
\& A.\,Pedlar$^1$ }}
$^1$ {Jodrell Bank Observatory, The University of Manchester, Macclesfield,
Cheshire, SK11 9DL, UK} \\
$^2$ {Harvard-Smithsonian Center for Astrophysics, SAO/SMA Project, P.O. Box 824,
Hilo, HI 9672, USA}\\
$^3$ {National Radio Astronomy Observatory, P.O. Box 1 Socorro, NM 87801, USA}\\
$^4$ {Istituto di Radioastronomia del CNR, via Gobetti 101, 40129 Bologna, Italy}
{We present new milliarcsecond resolution observations of the H{\sc i} absorption
against the kiloparsec scale inner jet of the radio galaxy 3C\,293. Using a
combination of observations obtained with global VLBI, MERLIN and the VLA we have
imaged the strong and extensive neutral hydrogen absorption against the radio
core and jet of this source across a wide range of angular scales.
In this proceedings we will present these new combined milliarcsecond scale VLBI
results alongside our previous lower resolution MERLIN studies of the H{\sc i}
absorption in this source. This study will allow us to investigate the
distribution and dynamics of the H{\sc i} absorption in the centre of this source
from scales of arcseconds to a few milliarcsecond.}
{To appear in the Proceedings of the 7th European VLBI Network Sympossium, Eds.
Rafael Bachiller, Francisco Colomer, Jean-Francois Desmurs, and Pablo de-Vicente}
{E-mail contact: rbeswick@jb.man.ac.uk,\newline preprint available at
http://www.jb.man.ac.uk/$\sim$rbeswick/papers/papers.html}
%%% ie. --> http://www.jb.man.ac.uk/~rbeswick/papers/papers.html
\newpage
{\large\bf{Transition (LINER/HII) nuclei as evolved Composite (Seyfert
2/Starburst) nuclei}}
{\bf{Thaisa Storchi-Bergmann$^1$,
C. H. Brandt$^1$, R. Cid Fernandes$^2$,
H. R. Schmitt$^3$, R. Gonz\'alez Delgado$^4$ }}
$^1$ {Instituto de F\'\i sica, UFRGS, Porto Alegre, RS, Brazil} \\
$^2$ {Departamento de F\'\i sica, CFM -- UFSC, Florian\'opolis, SC, Brazil}\\
$^3$ {National Radio Astronomy Observatory, Charlottesville, USA}\\
$^4$ {Instituto de Astrof\'\i sica de Andaluc\'\i a (CSIC), Granada, Spain}
{We compare the circumnuclear stellar population and environmental properies of
Seyfert and Composite (Seyfert + Starburst) nuclei with those of LINERs and
LINER/HII transition galaxies (TOs), and discuss evidence for evolution from
Seyfert/Composite to LINER/TO nuclei.}
{To appear in the Proceedings of IAU Symp. No. 222: the interplay among
Black Holes, Stars and ISM in Galactic Nuclei, CUP, Eds. T.
Storchi-Bergmann,
L. Ho and H. R. Schmitt}
{E-mail contact: thaisa@if.ufrgs.br,\newline preprint available at
http://arXiv.org/abs/astro-ph/0409729}
\vspace*{0.6cm}
{\large\bf{Probing the Kinematics of the Narrow-Line Region in Seyfert Galaxies
with Slitless Spectroscopy: Observational Results$^{1}$}}
{\bf
J.R. Ruiz$^{2}$,
D.M. Crenshaw$^{3}$,
S.B. Kraemer$^{2}$,
G.A. Bower$^{4}$,
T.R. Gull$^{5}$,
J.B. Hutchings$^{6}$,
M.E. Kaiser$^{7}$,
\& D. Weistrop$^{8}$}
$^{1}${Based on observations made with the NASA/ESA Hubble Space
Telescope, obtained at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS 5-26555. These
observations are associated with proposal GO-8340.}\\
$^{2}${Catholic University of America and Laboratory for Astronomy
and Solar Physics, NASA's Goddard Space Flight Center,
Code 681, Greenbelt, MD 20771; ruiz@yancey.gsfc.nasa.gov}\\
$^{3}${Department of Physics and Astronomy, Georgia State
University, Astronomy Offices, One Park Place South SE,
Suite 700, Atlanta, GA 30303; crenshaw@chara.gsu.edu}\\
$^{4}${Computer Sciences Corporation, Space Telescope Science
Institute, 3700 San Martin Drive, Baltimore, MD 21218}\\
$^{5}${Laboratory for Astronomy and Solar Physics, NASA's Goddard
Space Flight Center, Code 681, Greenbelt, MD 20771}\\
$^{6}${Dominion Astrophysical Observatory, National Research Council
of Canada, 5071 West Saanich Rd., Victoria, BC V9E 2E7,
Canada}\\
$^{7}${Department of Physics \& Astronomy, Johns Hopkins University,
3400 North Charles St., Baltimore, MD 21218}\\
$^{8}${Department of Physics, University of Nevada at Las Vegas,
4505 Maryland Parkway, Las Vegas, NV 89154-4002}
\def\arcsecpoint{$''\!.$}
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{
We present slitless spectra of 10 Seyfert galaxies observed with the Space
Telescope Imaging Spectrograph on the {\it Hubble Space Telescope} ({\it
HST}). The spectra cover the [O~III] $\lambda\lambda$4959, 5007 emission
lines at a spectral resolving power of $\lambda$/$\Delta\lambda$ $\approx$
9000 and a spatial resolution of $\sim$0\arcsecpoint1. We compare the slitless
spectra with previous {\it HST} narrow-band images to determine the velocity
shifts and dispersions of the bright emission-line knots in the narrow-line
regions (NLRs) of these Seyferts, which extend out to at least several hundred
pc from their nuclei. Many knots are spatially resolved with sizes of tenths
of arcsecs, corresponding to tens of pcs, and yet they appear to move
coherently with radial velocities between zero and $\pm$ 1200 km s$^{-1}$ with
respect to the systemic velocities of their host galaxies. The knots also show
a broad range in velocity dispersion, ranging from $\sim$30 km s$^{-1}$ (the
velocity resolution) to $\sim$1000 km s$^{-1}$ FWHM. Most of the Seyfert
galaxies in this sample show an organized flow pattern, with radial velocities
near zero at the nucleus (defined by the optical continuum peak) and
increasing to maximum blueshifts and redshifts within $\sim$ 1$''$ of the
nucleus, followed by a decline to the systemic velocity. However, there are
large local variations around this pattern and in one case (NGC~7212), the
radial velocities are nearly chaotic. The emission-line knots also follow a
general trend of decreasing velocity dispersion with increasing distance from
the nucleus. In the Seyfert 2 galaxies, the presence of blueshifts and
redshifts on either side of the nucleus indicates that rotation alone cannot
explain the observed radial velocities. The most straightforward
interpretation is that radial outflow plays an important role in the NLR
kinematics. Each of the Seyfert galaxies in this sample (with the exception of
Mrk 3) shows a bright, compact (FWHM $\leq$ 0\arcsecpoint5) [O III] knot at
the position of its optical nucleus. These nuclear emission-line knots have
radial-velocity centroids near zero, but they typically have the highest
velocity dispersions. Their similar properties suggest they may be a common,
distinct component of the NLR.}
{Accepted by The Astronomical Journal}
{E-mail contact: crenshaw@chara.gsu.edu,\newline preprint available at
http://arxiv.org/abs/astro-ph/0409754}
\newpage
\begin{center}
{\Large\sf Thesis}
\vspace*{0.6cm}
{\Large\bf{Linking the Power Sources of Emission-Line Galaxy Nuclei
from the Highest to the Lowest Redshifts}}
\vspace*{0.5cm}
{\bf{ Anca Constantin}}
{Thesis work conducted at: Department of Physics and Astronomy, Ohio
University, USA}
{Current address: Department of Physics, Drexel University, 3141
Chestnut Street, Philadelphia, PA 19104, USA}
{Electronic mail: constant@drexel.edu}
{Ph.D dissertation directed by: Joseph C. Shields}
{Ph.D degree awarded: August 2004}
\vspace*{0.8cm}
\end{center}
{This dissertation searches for common grounds for the diversity of properties
exhibited by the emission-line nuclei of galaxies, from large look-back times to
the local universe. I present results of (1) a program of high signal-to-noise
spectroscopy for 44 $z~^{>}_{\sim}~4$ quasars using the MMT and Keck
observatories; (2) a detailed analysis of the ultraviolet and optical spectral
behavior of 22 Narrow Line Seyfert 1 (NLS1) galaxies based on archival {\it
Hubble Space Telescope} (HST) spectra; (3) an in-depth investigation of the
proposed link between NLS1s and $z~^{>}_{\sim}~4$ quasars, by means of comparison
of composite spectra, and a Principal Component Analysis; (4) a simulation of
Seyferts/quasars designed to explore the role of dust in modifying their observed
spectral energy distribution; and (5) a sensitive search for accretion signatures
in a large sample of nearby emission-line galaxy nuclei, employing a quantitative
comparison of the nebular line flux ratios in small (HST) and large
(ground-based) apertures.
The low and high redshift quasars are found very similar in their emission
characteristics, although differences exist. In particular, the data bolster
indications of supersolar metallicities in the luminous, $z~^{>}_{\sim}~ 4$
sources, which support scenarios that assume substantial star formation
concurrent or preceding the quasar phenomena. Because high-$z$ sources are more
metal enriched and more spectroscopically heterogeneous than the NLS1s, a close
connection between these objects remains doubtful. The results show that NLS1s
have redder UV-blue continua than those measured in other quasars and Seyferts.
The sources with UV line absorption are in general less powerful and show redder
spectra, indicating that a luminosity-dependent dust absorption may be important
in modifying their continua. A receding-torus --like geometry seems to explain
these trends and other observed correlations between quasar luminosity and
continuum slope. Finally, in most of the nearby emission-line nuclei, the
expected increased AGN-like behavior at smaller scales is not seen, although the
nuclear emission is resolved. This suggests that these sources are not
necessarily powered by accretion onto a compact object, and that the composite
model proposed for the LINER/H {\sc II} transition nuclei (that assumes a central
accreting-type nucleus surrounded by star-forming regions) is not generally
supported.}
\vspace*{2.0cm}
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{
The Active Galaxies Newsletter is available on the World Wide Web.
You can access it via the University of Manchester home page :-
http://www.ast.man.ac.uk/$\sim$rb/agn/
%%% i.e. --> http://www.ast.man.ac.uk/~rb/agn/
\newline
If you move or your e-mail address changes, please send the editor
your new address. If the Newsletter repeatedly bounces back from an
address then that address is deleted from the mailing list.
}}}
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